As we already noted, the expected gamma-ray flux from DM annihilation is proportional to the so-called \(J\) -factor, which gives us information on how DM is distributed within the dSph (see Eq. REF  and Fig. REF ). In order to infer it, optical stellar-kinematic measurements are used such as the line-of-sight velocity and the position of stars potentially bound to the dSph  [1]}.
The \(J\)  factor is defined as:
\(\frac{dJ}{d\Omega }=\int _{los}\rho ^{2} (l,\Omega )dl\) 
